LAMOST LRS has a limiting magnitude of about 20 in \(g\)  band and its signal to noise ratio is higher than 6 on dark nights or 15 on bright nights. In MRS, the signal-to-noise ratio is always larger than 10. The parameters are given by the LAMOST Stellar Parameter pipeline (LASP), and their uncertainties are mainly from the stellar signal to noise ratio and chi-square of the best matched theoretical spectrum [1]}, [2]}. The parameter differences of the LRS data and MRS data are very small, on average 17.6 K for \(T_{\rm eff}\) , 0.028 dex for log \(g\)  (\(g\)  in \({\rm (cms^{-2})}\) ), and 0.084 dex for [Fe/H], according to our test. The internal uncertainties of LASP are estimated to be \(\Delta T_{\rm eff} \sim 80 \rm K \) , \(\Delta {\rm log} g \sim 0.15 \rm dex\) , and \(\Delta {\rm [Fe/H]} \sim 0.09 \rm dex\)  [3]}. We cross-match these catalogs with J-PLUS DR1 to within one arcsec using the Tool for OPerations on Catalogues And Tables (TOPCAT, [4]}). There are 216,114 and 25,170 cross-matched stars in the LRS and MRS catalogs, respectively.
